Direction - Conférence Extremely Large TelescopeLargeExtremely European The The E-ELT

• 40-m class : largest optical- infrared telescope in the world. • Segmented primary . • Active optics to maintain collimation and mirror figure. • assisted telescope. • Diffraction limited performance. • Wide field of view: 10 arcmin. • Mid-latitude site (Armazones in Chile). • Fast instrument changes. • VLT level of efficiency in operations. The Science • Contemporary science: Exoplanets: radial velocity detections, direct imaging, transit spectroscopy, proto-planetary disks Fundamental physics: GR in the strong field limit, variation of fundamental constants, expansion history of the Universe Resolved stellar populations: beyond the ALMA Local Group The physics of high-redshift galaxies …and much more! • Synergies with other top facilities: ALMA JWST LSST and other survey SKA LSST JWST • Discovery potential: Opening new parameter space in terms of spatial resolution and sensitivity

SKA The E-ELT Project

• Top priority of European ground-based astronomy (on Astronet and ESFRI lists). • Cerro Armazones in Chile selected as the E-ELT site in April 2010. • Detailed Design Phase completed in 2011. Construction Proposal published in Dec 2011. • Instrument Roadmap (Nov 2011): 2 first-light instruments + plan for 1st generation. • Project fully approved in Dec 2012. • Construction started in 2013. • Start of operations early next decade. • Construction cost: 1083 M€ (including first-light instrumentation). The Telescope

• Nasmyth telescope with a segmented M2: 4.2 m primary mirror. • Novel 5 mirror design to include M4 (AO): adaptive optics in the telescope. 2.4 m M5 (TT): • Classical 3 mirror anastigmat + 2 flat 2.6x2.1 m fold (M4, M5). M3: 3.8 m

Nasmyth focus M1 (seg): 39.3 m

• Two instrument platforms nearly the size of tennis courts can host 3 instruments each + Coudé lab. • Multiple laser guide stars, launched from the side. • Nearly 3000 tonnes of moving structure. The Mirrors M1: 39.3 m, 798 hexagonal segments of 1.45 m tip-to-tip: 978 m 2 collecting area

M4: 2.4 m, flat, adaptive 6000 to 8000 actuators

M5: 2.6 x 2.1 m, flat, provides tip-tilt correction The Instruments

• The telescope can host eight instruments. • 2007 – 2010: eight instrument and two adaptive optics module concept studies were conducted by the community.

• Instrument Roadmap (2011): The Site

Armazones

Paranal More information

The science users web pages: www.eso.org/sci/facilities/eelt

The E-ELT Construction Proposal: www.eso.org/sci/facilities/eelt/docs/eelt_constrproposal.pdf The E-ELT Science Case: www.eso.org/sci/facilities/eelt/science/doc/eelt_sciencecase.pdf

The E-ELT Design Reference Mission: www.eso.org/sci/facilities/eelt/science/doc/drm_report.pdf

The public web pages: www.eso.org/public/telesinstr/eelt.html

Brochures, Posters, etc: www.eso.org/public/products/brochures/

Gallery: www.eso.org/public/images/archive/category/eelt/ Direction - Conférence Lessons Adaptive Optics for for Ican Optics Department, Onera Department, Optics Vincent Michau & Cophasing& : Direction - Conférence dpieOtc (AO)Optics Adaptive Direction - Conférence ICAN cophasing ICAN cophasing byAO an architecture guyseen control control unit φ hasePh φ High WFSrateHigh splitter Beam Compressor Combiner Control system Control system Beam + o rateWFS Low splitter Beam Direction - Conférence Adaptive Optics Adaptive Direction - Conférence AO architecturecontrol system Sensor WFS WFS area Signal Video reduction Data Control system Control Meas. WFS processing Control HT Voltages Direction - Conférence • • • AO systems for E-ELT(39m) Preliminary designsPreliminary Sampling frequency: 500 Hz Hz 500 frequency:Sampling actuators 7000 mirror: Deformable measurements 15000 WFS: 84x84 84x84 sub-apertures ICAN cophasing system ICANcophasing Sampling frequency: 100 Hz Hz 100 frequency:Sampling measurements 20000 units 10000 : control Phase WFS: 15 Direction - Conférence Complexity Control Optics Adaptive Number of operations/T s & Computing Efficient Solutions Efficient &Computing 10 10 10 10 10 10 10 0 2 4 6 8 10 12 10 0 FFT FFT based control Matrixbased control 10 1 Number of degrees-of-freedom NAOS ∝ ∝ VLT 10 Scaling Scaling laws Nact 2 Nact log(Nact) 2 SAXO SAXO VL T+ 10 3 ELT SCAO-ELT Nact 10 4 ICAN 10 5 (turbulence, vibrations...) (turbulence, perturbation on priors temporal and spatial to thanks performance better Gaussian Quadratic Linear • integrator• strategies:control of Choice approximations sparse FFTor • equationsmatrix general • formulation:problem of Choice (based (based on Kalman filter) Direction - Conférence Complexity Control Optics Adaptive

Number of operations/Ts & Computing Efficient Solutions Efficient &Computing • • : Onera of Position 10 10 10 10 10 10 10 6 8 10 12 0 2 4 10 (SPHERE/ SAXO) (SPHERE/ co of calibrationand implementation Specification, design, System 0 FFT FFT based control Matrixbased control 10 1 Number of degrees-of-freedom NAOS ∝ ∝ 10 Scaling Scaling laws Nact 2 Nact log(Nact) 2 SAXO SAXO 10 3 SCAO-ELT Nact ICAN 10 4 10 5 • Development of spatially spatially of Development • spatial 2D point-to-point fast Ultra • on based solutions Iterative • Computational complexity brought complexity Computational ntrol on operational systems operationalon ntrol down to O(n log n) or even O(n) even or log n) O(n to down (LAM/Onera): solution LQG distributed (IOGS/Onera) LQG as such solutions control optimal of Acceleration (Austria) wavefront of integration gradient conjugated preconditioned nr among few leading institutesOnera in adaptive optics control research Direction - Conférence Conclusion • • design design and new developments for AO control for ELT ICAN may take advantage of experience in AO loop number of degrees of freedom (ELT, ICAN …) Control is a major issue for systems with very large • • • Calibration Calibration and identification Hardware and software architecture Algorithms • • Direction• -Sphere Conférence Cooperation : Grenoble, Marseille, Geneva, Zurick, AO:1371 actuators, f = 1200 Hz) + cor XAO(eXtreme Detection of Jupiter like exoplanets aoaosraois PA() srn(NL) observatories, MPIA (D), Astron Padova ngah+ differential spectral imagingonograph